New form of dynamo equation for convective regions of rotating stars

Details New form of dynamo equation for convective regions of rotating stars New form of dynamo equation for convective regions of rotating stars

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992ap%26ss.189..147b&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 189, no. 1, March 1992, p. 147-149.

Astronomy and Astrophysics

Astrophysics

1

Convective Flow, Dynamo Theory, Stellar Rotation, Mixing Length Flow Theory, Stellar Magnetic Fields, Turbulence Effects, Viscosity

Scientific paper

Differential rotation generated by convection in rotating stars leads to amplification of the toroidal magnetic field. As there is a direct connection between rotational velocity ~»= and its gradient V~, the equation of magnetic field generation contains terms, depending directly on ~. It follows, therefore, that the mechanism of the ~ - w dynamo is always realized in convective zones of stationary rotating stars making the action of the ~2-dynamo unimportant

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